Past political open doors : Intercosmos 1967 no dispatch installments

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SphinX will gauge total component plenitudes utilizing line highlights because of neon, ... SphinX will likewise concentrate calm coronal warming procedures through photon ...

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Past political open doors : Intercosmos 1967 no dispatch installments Plesetsk Orbital missions 3 dispatches 1994 Coronas-I 1995 Interball-Tail 2001 Coronas-F Kapustin Yar Sounding rockets 7 dispatches 1970 1971 1977 1979 1980 1981 1983 1984

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The First Polish Space analyze Pin-gap cameras

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The Team: PI Janusz Sylwester SphinX delicate X-beam spectrophotometer Mirek Kowalinski : Project Manager Jarek Bakała : Project Constructor Szymon Gburek: Project Scientist Marek Siarkowski, Barbara Sylwester, Zbigniew Kordylewski, Piotr Podgórski, Witold Trzebiński, Stefan Płocieniak , Anna Kępa FIAN: Dr. Sergey Kuzin, TESIS PI MEPhI : Yury Kotov , CORONAS-Photon PM AI CzAS : Dr. Franta Farnik Prof. Fabio Reale, INAFA, Palermo University Prof. Ken Phillips, UCL, London

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CORONAS-F dispatch, circle & guiding 31 July 2001, polar circle, 95min, ~500 km semi-Sun-synchronous SS-14 Cyclone x 10 , CORONAS-F

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Satellite CORONAS-PHOTON TESIS SphinX STEP-F KONUS-RF-hostile to weight vessel PHOKA RT-2/GA RT-2/S KONUS-RF N-2M RT-2/G PINGUIN Magnetometer Launch is settled toward the most recent week of 2008 !

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Full Solar circle UV & delicate X-beam screens

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TESIS get together of instruments for XUV imaging spectroscopy of the Sun It is propelled variant of the SPIRIT instrument

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SphinX & TESIS SphinX

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Instruments for charge molecule estimations 3-hub magnetometer

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SphinX development EUV channels ( doubly aluminized Mylar ) Photometer Collimators (+-2.5 deg ) Three openings D1, D2, D3 Shutter Stepper engine FFU Filters Targets D4 Electronics Front end Amptek Digital „ our " Controller Software reinventing Heat sink Alignment reflect

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Measurement channels P h o t o m e t r i c FFU D2 D1 D3 D4 φ : 5 mm A: 13.0 mm 2 8 μ s Up to 60 000 cts/s FWHM: 490 eV φ : 4 mm A: 0.26 mm 2 25 μ s Up to 20 000 cts/s FWHM: 290 eV φ : 4 mm A: 0.0052 mm 2 25 μ s Up to 20 000 cts/s FWHM: 290 eV φ : 4 mm A: 13.0 mm 2 25 μ s Up to 20 000 cts/s FWHM: 290 eV $4000 Detectors (four units): 256/1024 vitality canisters Amptek , Peltier cooled (- 50 deg ) Si PIN diodes. Identifiers' bolster plate thermally associated with outer warmth radiator by means of warmth sink pipe. Photon entry time measured to inside 2 μs (in Time Stamping Mode ) Much preferred vitality determination over gas finders 2.5 % against 16% , low warm clamor

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Expected aggregate number rates Courtesy; Marek Siarkowski

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SphinX adjustment BESSY synchrotron Berlin February 26th 2008 March second 2008 D3 RAS Meeting 9 May 2008 Janusz Sylwester, Poland : Ongoing and future sun powered X-beam testing

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How it looks from the tests The BESSY synchrotron input range ( red ) with overplotted reaction of SphinX D2 identifier ( dark ). Ostensible successful territories have been utilized. The understanding is superior to anything 5% in the vitality band where SphinX locators are the most delicate. BESSY Berlin Synchrotron: - All indicator linearity: consummate (0.1% ) more than 0.8-14.5 keV ; dynamic range 10 4 . - total reaction known to superior to anything 5% against reference synchrotron source. - heap up matri c es known as measured from X-beam 4 gem monochromator spectra got at 8 energies somewhere around 1.5 and 8 keV

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The estimation environment, bcgd: ~few cts/s up to 10 3 cts/s (SAA) SAA Night RB Night Flare CORONAS-F Important pahases S/C X-beam day S/C optical day S/C optical night S/C X-beam night Terminator crossing Previous CORONAS-F circle

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Time stamping mode D1, D2 or D3 rates < 10 3/s Time stamping mode from : D1, D2, D3, D4 2 Bytes for processor time of the identifier occasion begin 1 byte for the sufficiency Allows to decide the distinction between occasions to inside 2 μ s ~2/1000 exactness Absolute planning to inside 0.001s against UT Expected rates D1= 10 3 occasions/s ( occasion : Amplitude 1byte, time 2 bytes )- 3 KB/s D2= 10 occasions/s, D3= 10 occasions/s, D4= 10 occasions/s Total: 3Kbytes/s – can keep going for ~10000s (3 h) every dump – may cover 100% cycle with pressure

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Waiting time investigation – is the procedure at low tally rate Poissonian? Wheatland, The Astrophysical Journal, Volume 679, Issue 2, pp. 1621-1628 , 2008 Radioactive sources give a perfect case of the measurements To what degree the entry times of photons from the „ calm " crown have „no memory " i.e they have the exponential holding up time dissemination ? ( Models for flare measurements accept or foresee that flares are free occasions - however this is under question ) The essential errand for the underlying part of the mission where the action is relied upon to be low .

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SphinX convolved spectra (A coronal ) O, Ne,Fe Shape relies on upon T Si Ca Ar Fe S Ni Fe Ni 25 MK unadulterated continuum 10 MK 5 MK

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Predicted conduct of movement amid dynamic period of Coronas-Photon

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Energy Calibration D1,D2,D3 sunlight based initiated fluorescence spectra of immaculate components During flares ~> M1 Until 10^6 cts gathered for every finder Approximately every month If v. calm condition then on the charge from the beginning 10 min

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Terminator travel: Profile of Earth atmospecric retention X-beam eliminator crossing calculation operational on load up Predict the passage/exit to inside few moments Spectra 256 vitality canisters each 0.1 sec give no less than 1 km determination in the vertical Earth assimilation profile Time stamping or phantom mode relying upon the flare signal

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SphinX firsts SphinX will quantify outright component plenitudes utilizing line highlights because of neon, magnesium, silicon, sulfur , argon, calcium, iron and nickel in different levels of sun powered movement (calm Sun, dynamic districts and flares). It ought to in this manner be in a solid position to give an authoritative response to the proceeding with verbal confrontation about the reliance of coronal plenitudes of components on their first ionization potential, the purported FIP impact. SphinX will get the primary completely aligned sun oriented X-beam spectra in the 0.8- - 15 keV go . Specifically this will help us to comprehend the RHESSI continuum perceptions in this troublesome range. SphinX will likewise concentrate calm coronal warming procedures through photon landing time- - distanc e examination (the entry time of a X-beam photon will be measured to a few microseconds); X-beam motions in the <1 to 500 s period range; and transient ionization in flares.

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Instrument satus Flight demonstrate at the Moscow „factory" experiencing last electro-attractive & teelmetry similarity tests On November 30, TESIS ( a mother instrument for SphinX) is wanting a last support tests to FIAN (MK+WT) will reload the flight program The Coronas-Photon dispatch is normal before the end of 2008 a X-mas display? Ground division of programming v1 prepared (Czech commitment under direction od Szymon) 2 reflect servers (Wrocław, Ondrejov) Automatic information access to FIAN SphinX information stream (~12 hours greatest deferral if 2 dumps/24h) Automatic lessening to Level2 Data distributed to the community territory (90% information will go there choice taken by the obligation researcher) Automatic flare occasion inventory creation start,max, end, class, Tmax, Emmax, rise stage dur L, H, EMmax-Tmax postpone Auxiliary information accessible: GOES, RHESSI, SOXS

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The FFU unit (channel fluorescence unit) Filter-Fluorescence Unit (FFU) format This unit will be dynamic constantly: time stamping < 1000 cts/s or spectra (256 containers)